Towards a unified model for black hole X-ray binary jets

Fender, R. P.; Belloni, T.; Gallo, Elena

doi:10.1111/j.1365-2966.2004.08384.x

Cited by 1,309 publications

(1,809 citation statements)

References 105 publications

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“…Relativistic transient jets are usually observed in the hardto-soft transition (Fender, Belloni & Gallo 2004;RM06), and a correlation between jet power and BH spin was discovered for five BHXBs, which means that the transient jets are powered by extracting rotational energy of BH probably via the BZ process (Blandford & Znajek 1977;Narayan & McClintock 2012;McClintock & Narayan 2013). It is noticed that both the 3:2 HFQPO pairs and the relativistic transient jets are observed in the hard-to-soft state transitions of the four sources, GRO J1655−40, XTE J1550−564, GRS 1915+105 and H1743−322.…”

Section: Discussionmentioning

confidence: 99%

A model for 3:2 HFQPO pairs in black hole binaries based on cosmic battery

Huang¹,

Ye²,

Wang³

et al. 2016

Mon. Not. R. Astron. Soc.

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A model for 3:2 high-frequency quasi-periodic oscillations (HFQPOs) with 3:2 pairs observed in four black hole X-ray binaries (BHXBs) is proposed by invoking the epicyclic resonances with the magnetic connection (MC) between a spinning black hole (BH) with a relativistic accretion disc. It turns out that the MC can be worked out due to Poynting-Robertson cosmic battery (PRCB), and the 3:2 HFQPO pairs associated with the steep power-law states can be fitted in this model. Furthermore, the severe damping problem in the epicyclic resonance model can be overcome by transferring energy from the BH to the inner disc via the MC process for emitting X-rays with sufficient amplitude and coherence to produce the HFQPOs. In addition, we discuss the important role of the magnetic field in state transition of BHXBs.

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Section: Discussionmentioning

confidence: 99%

A model for 3:2 HFQPO pairs in black hole binaries based on cosmic battery

Huang¹,

Ye²,

Wang³

et al. 2016

Mon. Not. R. Astron. Soc.

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“…Its location is close to that of the HIMS-SIMS transition (which is defined by marked and abrupt changes in the timing properties, see Belloni 2010), although an exact correspondence could not be made with the current data, rather sparse in radio (Fender et al 2009). It also marks the disappearance of the compact jet (see Fender et al 2004;Miller-Jones et al 2012). As discussed in Kylafis et al (2012), at this stage the geometrically thin disk is not able to sustain the magnetic field produced by the PRCB and becomes unstable to non-axisymmetric "Rayleigh-Taylortype" instability modes.…”

Section: First Jet-line Crossingmentioning

confidence: 98%

Accretion and Ejection in Black-Hole X-Ray Transients

Kylafis

Belloni

2014

The Formation and Disruption of Black Hole Jets

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Context. A rich phenomenology has been accumulated over the years regarding accretion and ejection in black-hole X-ray transients (BHTs) and it needs an interpretation. Aims. Here we summarize the current observational picture of the outbursts of BHTs, based on the evolution traced in a hardness -luminosity diagram (HLD), and we offer a physical interpretation. Methods. The basic ingredient in our interpretation is the Poynting -Robertson Cosmic Battery (PRCB, Contopoulos & Kazanas 1998), which provides locally the poloidal magnetic field needed for the ejection of the jet. In addition, we make two assumptions, easily justifiable. The first is that the mass-accretion rate to the black hole in a BHT outburst has a generic bell-shaped form, whose characteristic time scale is much longer than the dynamical or the cooling ones. This is guaranteed by the observational fact that all BHTs start their outburst and end it at the quiescent state, i.e., at very low accretion rate, and that state transitions take place over long time scales (hours to days). The second assumption is that at low accretion rates the accretion flow is geometrically thick, ADAF-like, while at high accretion rates it is geometrically thin. Last, but not least, we demonstrate that the previous history of the system is absolutely necessary for the interpretation of the HLD. Results. Both, at the beginning and the end of an outburst, the PRCB establishes a strong poloidal magnetic field in the ADAF-like part of the accretion flow, and this explains naturally why a jet is always present in the right part of the HLD. In the left part of the HLD, the accretion flow is in the form of a thin disk, and such a disk cannot sustain a strong poloidal magnetic filed. Thus, no jet is expected in this part of the HLD. Finally, the counterclockwise traversal of the HLD is explained as follows: all outbursts start from the quiescent state, in which the inner part of the accretion flow is ADAF-like, threaded by a poloidal magnetic field. As the accretion rate increases and the source moves to the hard state, the poloidal magnetic field in the ADAF forces the flow to remain ADAF and the source to move upwards in the HLD rather than to turn left. Thus, the history of the system determines the counterclockwise traversal of the HLD. As a result, no BHT is expected to ever traverse the entire HLD curve in the clockwise direction. Conclusions. We offer a physical interpretation of accretion and ejection in BHTs with only one parameter, the mass transfer rate, plus the history of the system.

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“…From the combined analysis of the EPIC-pn and MOS2 data we find the flux of the disk blackbody component to be ∼ 5 times lower than that of the power law component in the 1.2 − 10 keV range. The strong and hard (Γ ∼ 1.50) (EPIC-pn) powerlaw and a weak disk component are typical of black hole X-ray binaries in the hard state (see e.g., Belloni et al 2002a;Fender et al 2004;Remillard & McClintock 2006).…”

Section: Discussionmentioning

confidence: 99%

XMM–Newton view of a hard X-ray transient IGR J17497–2821

Alam

Mukherjee

Mondal

et al. 2015

Monthly Notices of the Royal Astronomical Society

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We present spectral and energy dependent timing characteristics of the hard X-ray transient IGR J17497-2821 based on XMM-Newton observations performed five and nine days after its outburst on 2006 September 17. We find that the source spectra can be well described by a hard (Γ ∼ 1.50) powerlaw and a weak multicolour disk blackbody with inner disk temperature kT in ∼ 0.2 keV. A broad iron Kα line with FWHM∼ 27000 km s −1 , consistent with that arising from an accretion disk truncated at large radius, was also detected. The power density spectra of IGR J17497-2821, derived from the high resolution (30µs) timing mode XMM-Newton observations, are characterised by broadband noise components that are well modelled by three Lorentzians. The shallow power law slope, low disk luminosity and the shape of the broadband power density spectrum indicate that the source was in the hard state. The rms variability in the softer energy bands (0.3 − 2 keV) found to be ∼ 1.3 times that in 2 − 5 and 5 − 10 keV energy bands. We also present the energy dependent timing analysis of the RXTE/PCA data, where we find that at higher energies, the rms variability increases with energy.

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Towards a unified model for black hole X-ray binary jets

Cited by 1,309 publications

References 105 publications

A model for 3:2 HFQPO pairs in black hole binaries based on cosmic battery

A model for 3:2 HFQPO pairs in black hole binaries based on cosmic battery

Accretion and Ejection in Black-Hole X-Ray Transients

XMM–Newton view of a hard X-ray transient IGR J17497–2821

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